The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta

Autores: Nicholl, M.; Berger, E.; Kasen, D.; Metzger, B. D.; Elias, J.; Briceño, C.; Alexander, K. D.; Blanchard, P. K.; Chornock, R.; Cowperthwaite, P. S.; Eftekhari, T.; Fong, W.; Margutti, R.; Villar, V. A.; Williams, P. K. G.; Brown, W.; Annis, J.; Bahramian, A.; Brout, D.; Brown, D. A.; Chen, H. Y.; Clemens, J.C.; Dennihy, E.; Dunlap, B.; Holz, D.E.; Marchesini, Ezequiel Joaquín; Massaro, F.; Moskowitz, N.; Pelisoli, I.; Rest, A.; Ricci, F.; Sako, M.; Soares Santos, M.; Strader, J.
Año de publicación: 2017
Idioma: inglés
Tipo de recurso: artículo
Estado: versión publicada
Descripción: We present optical and ultraviolet spectra of the first electromagnetic counterpart to a gravitational-wave (GW) source, the binary neutron star merger GW170817. Spectra were obtained nightly between 1.5 and 9.5 days post-merger, using the Southern Astrophysical Research and Magellan telescopes; the UV spectrum was obtained with the Hubble Space Telescope at 5.5 days. Our data reveal a rapidly fading blue component (T ≈ 5500 K at 1.5 days) that quickly reddens; spectra later than ≳4.5 days peak beyond the optical regime. The spectra are mostly featureless, although we identify a possible weak emission line at ∼7900 Å; at t ≲ 4.5 days. The colors, rapid evolution, and featureless spectrum are consistent with a "blue" kilonova from polar ejecta comprised mainly of light r-process nuclei with atomic mass number A ≲ 140. This indicates a sightline within θobs ≲ 45° of the orbital axis. Comparison to models suggests ∼0.03 M o of blue ejecta, with a velocity of . The required lanthanide fraction is ∼10-4, but this drops to <10-5in the outermost ejecta. The large velocities point to a dynamical origin, rather than a disk wind, for this blue component, suggesting that both binary constituents are neutron stars (as opposed to a binary consisting of a neutron star and a black hole). For dynamical ejecta, the high mass favors a small neutron star radius of ≲12 km. This mass also supports the idea that neutron star mergers are a major contributor to r-process nucleosynthesis.
Fil: Nicholl, M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Berger, E.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Kasen, D.. Lawrence Berkeley National Laboratory; Estados Unidos. University of California at Berkeley; Estados Unidos
Fil: Metzger, B. D.. Columbia University In The City Of New York; Estados Unidos
Fil: Elias, J.. Southern Astrophysical Research Telescope; Chile
Fil: Briceño, C.. Cerro Tololo Inter American Observatory; Chile
Fil: Alexander, K. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Blanchard, P. K.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Chornock, R.. Ohio University; Estados Unidos
Fil: Cowperthwaite, P. S.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Eftekhari, T.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Fong, W.. Northwestern University; Estados Unidos
Fil: Margutti, R.. Northwestern University; Estados Unidos
Fil: Villar, V. A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Williams, P. K. G.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Brown, W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Annis, J.. Fermi National Accelerator Laboratory; Estados Unidos
Fil: Bahramian, A.. Michigan State University; Estados Unidos
Fil: Brout, D.. University of Pennsylvania; Estados Unidos
Fil: Brown, D. A.. Syracuse University; Estados Unidos
Fil: Chen, H. Y.. University of Chicago; Estados Unidos
Fil: Clemens, J.C.. University of North Carolina; Estados Unidos
Fil: Dennihy, E.. University of North Carolina; Estados Unidos
Fil: Dunlap, B.. University of North Carolina; Estados Unidos
Fil: Holz, D.E.. University of Chicago; Estados Unidos
Fil: Marchesini, Ezequiel Joaquín. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica; Italia. Istituto Nazionale Di Fisica Nucleare; Italia. Università di Torino; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Física de Líquidos y Sistemas Biológicos. Universidad Nacional de La Plata. Facultad de Ciencias Exactas. Instituto de Física de Líquidos y Sistemas Biológicos; Argentina
Fil: Massaro, F.. Istituto Nazionale Di Fisica Nucleare; Italia. Istituto Nazionale Di Astrofisica; Italia. Università di Torino; Italia
Fil: Moskowitz, N.. Lowell Observatory; Estados Unidos
Fil: Pelisoli, I.. Universidade Federal do Rio Grande do Sul; Brasil. University of Warwick; Reino Unido
Fil: Rest, A.. Space Telescope Science Institute; Estados Unidos. University Johns Hopkins; Estados Unidos
Fil: Ricci, F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Universita Degli Studi Roma Tre; Italia
Fil: Sako, M.. University of Pennsylvania; Estados Unidos
Fil: Soares Santos, M.. Fermi National Accelerator Laboratory; Estados Unidos. Brandeis University; Estados Unidos
Fil: Strader, J.. Michigan State University; Estados Unidos
Materia: BINARIES: CLOSE
GRAVITATIONAL WAVES
NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES
STARS: NEUTRON
Nivel de accesibilidad: acceso abierto
Condiciones de uso: https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
Institución: Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador: oai:ri.conicet.gov.ar:11336/56893

Acceder

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spelling	The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar EjectaNicholl, M.Berger, E.Kasen, D.Metzger, B. D.Elias, J.Briceño, C.Alexander, K. D.Blanchard, P. K.Chornock, R.Cowperthwaite, P. S.Eftekhari, T.Fong, W.Margutti, R.Villar, V. A.Williams, P. K. G.Brown, W.Annis, J.Bahramian, A.Brout, D.Brown, D. A.Chen, H. Y.Clemens, J.C.Dennihy, E.Dunlap, B.Holz, D.E.Marchesini, Ezequiel JoaquínMassaro, F.Moskowitz, N.Pelisoli, I.Rest, A.Ricci, F.Sako, M.Soares Santos, M.Strader, J.BINARIES: CLOSEGRAVITATIONAL WAVESNUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCESSTARS: NEUTRONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present optical and ultraviolet spectra of the first electromagnetic counterpart to a gravitational-wave (GW) source, the binary neutron star merger GW170817. Spectra were obtained nightly between 1.5 and 9.5 days post-merger, using the Southern Astrophysical Research and Magellan telescopes; the UV spectrum was obtained with the Hubble Space Telescope at 5.5 days. Our data reveal a rapidly fading blue component (T ≈ 5500 K at 1.5 days) that quickly reddens; spectra later than ≳4.5 days peak beyond the optical regime. The spectra are mostly featureless, although we identify a possible weak emission line at ∼7900 Å; at t ≲ 4.5 days. The colors, rapid evolution, and featureless spectrum are consistent with a "blue" kilonova from polar ejecta comprised mainly of light r-process nuclei with atomic mass number A ≲ 140. This indicates a sightline within θobs ≲ 45° of the orbital axis. Comparison to models suggests ∼0.03 M o of blue ejecta, with a velocity of . The required lanthanide fraction is ∼10-4, but this drops to <10-5in the outermost ejecta. The large velocities point to a dynamical origin, rather than a disk wind, for this blue component, suggesting that both binary constituents are neutron stars (as opposed to a binary consisting of a neutron star and a black hole). For dynamical ejecta, the high mass favors a small neutron star radius of ≲12 km. This mass also supports the idea that neutron star mergers are a major contributor to r-process nucleosynthesis.Fil: Nicholl, M.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Berger, E.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Kasen, D.. Lawrence Berkeley National Laboratory; Estados Unidos. University of California at Berkeley; Estados UnidosFil: Metzger, B. D.. Columbia University In The City Of New York; Estados UnidosFil: Elias, J.. Southern Astrophysical Research Telescope; ChileFil: Briceño, C.. Cerro Tololo Inter American Observatory; ChileFil: Alexander, K. D.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Blanchard, P. K.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Chornock, R.. Ohio University; Estados UnidosFil: Cowperthwaite, P. S.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Eftekhari, T.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Fong, W.. Northwestern University; Estados UnidosFil: Margutti, R.. Northwestern University; Estados UnidosFil: Villar, V. A.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Williams, P. K. G.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Brown, W.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Annis, J.. Fermi National Accelerator Laboratory; Estados UnidosFil: Bahramian, A.. Michigan State University; Estados UnidosFil: Brout, D.. University of Pennsylvania; Estados UnidosFil: Brown, D. A.. Syracuse University; Estados UnidosFil: Chen, H. Y.. University of Chicago; Estados UnidosFil: Clemens, J.C.. University of North Carolina; Estados UnidosFil: Dennihy, E.. University of North Carolina; Estados UnidosFil: Dunlap, B.. University of North Carolina; Estados UnidosFil: Holz, D.E.. University of Chicago; Estados UnidosFil: Marchesini, Ezequiel Joaquín. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica; Italia. Istituto Nazionale Di Fisica Nucleare; Italia. Università di Torino; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Física de Líquidos y Sistemas Biológicos. Universidad Nacional de La Plata. Facultad de Ciencias Exactas. Instituto de Física de Líquidos y Sistemas Biológicos; ArgentinaFil: Massaro, F.. Istituto Nazionale Di Fisica Nucleare; Italia. Istituto Nazionale Di Astrofisica; Italia. Università di Torino; ItaliaFil: Moskowitz, N.. Lowell Observatory; Estados UnidosFil: Pelisoli, I.. Universidade Federal do Rio Grande do Sul; Brasil. University of Warwick; Reino UnidoFil: Rest, A.. Space Telescope Science Institute; Estados Unidos. University Johns Hopkins; Estados UnidosFil: Ricci, F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Universita Degli Studi Roma Tre; ItaliaFil: Sako, M.. University of Pennsylvania; Estados UnidosFil: Soares Santos, M.. Fermi National Accelerator Laboratory; Estados Unidos. Brandeis University; Estados UnidosFil: Strader, J.. Michigan State University; Estados UnidosInstitute of Physics Publishing2017-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/56893Nicholl, M.; Berger, E.; Kasen, D.; Metzger, B. D.; Elias, J.; et al.; The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta; Institute of Physics Publishing; Astrophysical Journal Letters; 848; 2; 10-2017; 1-82041-8213CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/2041-8213/aa9029info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/2041-8213/aa9029/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:31:57Zoai:ri.conicet.gov.ar:11336/56893instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 11:31:57.508CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv	The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta
title	The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta
spellingShingle	The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta Nicholl, M. BINARIES: CLOSE GRAVITATIONAL WAVES NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES STARS: NEUTRON
title_short	The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta
title_full	The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta
title_fullStr	The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta
title_full_unstemmed	The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta
title_sort	The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta
dc.creator.none.fl_str_mv	Nicholl, M. Berger, E. Kasen, D. Metzger, B. D. Elias, J. Briceño, C. Alexander, K. D. Blanchard, P. K. Chornock, R. Cowperthwaite, P. S. Eftekhari, T. Fong, W. Margutti, R. Villar, V. A. Williams, P. K. G. Brown, W. Annis, J. Bahramian, A. Brout, D. Brown, D. A. Chen, H. Y. Clemens, J.C. Dennihy, E. Dunlap, B. Holz, D.E. Marchesini, Ezequiel Joaquín Massaro, F. Moskowitz, N. Pelisoli, I. Rest, A. Ricci, F. Sako, M. Soares Santos, M. Strader, J.
author	Nicholl, M.
author_facet	Nicholl, M. Berger, E. Kasen, D. Metzger, B. D. Elias, J. Briceño, C. Alexander, K. D. Blanchard, P. K. Chornock, R. Cowperthwaite, P. S. Eftekhari, T. Fong, W. Margutti, R. Villar, V. A. Williams, P. K. G. Brown, W. Annis, J. Bahramian, A. Brout, D. Brown, D. A. Chen, H. Y. Clemens, J.C. Dennihy, E. Dunlap, B. Holz, D.E. Marchesini, Ezequiel Joaquín Massaro, F. Moskowitz, N. Pelisoli, I. Rest, A. Ricci, F. Sako, M. Soares Santos, M. Strader, J.
author_role	author
author2	Berger, E. Kasen, D. Metzger, B. D. Elias, J. Briceño, C. Alexander, K. D. Blanchard, P. K. Chornock, R. Cowperthwaite, P. S. Eftekhari, T. Fong, W. Margutti, R. Villar, V. A. Williams, P. K. G. Brown, W. Annis, J. Bahramian, A. Brout, D. Brown, D. A. Chen, H. Y. Clemens, J.C. Dennihy, E. Dunlap, B. Holz, D.E. Marchesini, Ezequiel Joaquín Massaro, F. Moskowitz, N. Pelisoli, I. Rest, A. Ricci, F. Sako, M. Soares Santos, M. Strader, J.
author2_role	author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author
dc.subject.none.fl_str_mv	BINARIES: CLOSE GRAVITATIONAL WAVES NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES STARS: NEUTRON
topic	BINARIES: CLOSE GRAVITATIONAL WAVES NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES STARS: NEUTRON
purl_subject.fl_str_mv	https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv	We present optical and ultraviolet spectra of the first electromagnetic counterpart to a gravitational-wave (GW) source, the binary neutron star merger GW170817. Spectra were obtained nightly between 1.5 and 9.5 days post-merger, using the Southern Astrophysical Research and Magellan telescopes; the UV spectrum was obtained with the Hubble Space Telescope at 5.5 days. Our data reveal a rapidly fading blue component (T ≈ 5500 K at 1.5 days) that quickly reddens; spectra later than ≳4.5 days peak beyond the optical regime. The spectra are mostly featureless, although we identify a possible weak emission line at ∼7900 Å; at t ≲ 4.5 days. The colors, rapid evolution, and featureless spectrum are consistent with a "blue" kilonova from polar ejecta comprised mainly of light r-process nuclei with atomic mass number A ≲ 140. This indicates a sightline within θobs ≲ 45° of the orbital axis. Comparison to models suggests ∼0.03 M o of blue ejecta, with a velocity of . The required lanthanide fraction is ∼10-4, but this drops to <10-5in the outermost ejecta. The large velocities point to a dynamical origin, rather than a disk wind, for this blue component, suggesting that both binary constituents are neutron stars (as opposed to a binary consisting of a neutron star and a black hole). For dynamical ejecta, the high mass favors a small neutron star radius of ≲12 km. This mass also supports the idea that neutron star mergers are a major contributor to r-process nucleosynthesis. Fil: Nicholl, M.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Berger, E.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Kasen, D.. Lawrence Berkeley National Laboratory; Estados Unidos. University of California at Berkeley; Estados Unidos Fil: Metzger, B. D.. Columbia University In The City Of New York; Estados Unidos Fil: Elias, J.. Southern Astrophysical Research Telescope; Chile Fil: Briceño, C.. Cerro Tololo Inter American Observatory; Chile Fil: Alexander, K. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Blanchard, P. K.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Chornock, R.. Ohio University; Estados Unidos Fil: Cowperthwaite, P. S.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Eftekhari, T.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Fong, W.. Northwestern University; Estados Unidos Fil: Margutti, R.. Northwestern University; Estados Unidos Fil: Villar, V. A.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Williams, P. K. G.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Brown, W.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Annis, J.. Fermi National Accelerator Laboratory; Estados Unidos Fil: Bahramian, A.. Michigan State University; Estados Unidos Fil: Brout, D.. University of Pennsylvania; Estados Unidos Fil: Brown, D. A.. Syracuse University; Estados Unidos Fil: Chen, H. Y.. University of Chicago; Estados Unidos Fil: Clemens, J.C.. University of North Carolina; Estados Unidos Fil: Dennihy, E.. University of North Carolina; Estados Unidos Fil: Dunlap, B.. University of North Carolina; Estados Unidos Fil: Holz, D.E.. University of Chicago; Estados Unidos Fil: Marchesini, Ezequiel Joaquín. Inaf Istituto Di Astrofisica Spaziale E Fisica Cosmica; Italia. Istituto Nazionale Di Fisica Nucleare; Italia. Università di Torino; Italia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Física de Líquidos y Sistemas Biológicos. Universidad Nacional de La Plata. Facultad de Ciencias Exactas. Instituto de Física de Líquidos y Sistemas Biológicos; Argentina Fil: Massaro, F.. Istituto Nazionale Di Fisica Nucleare; Italia. Istituto Nazionale Di Astrofisica; Italia. Università di Torino; Italia Fil: Moskowitz, N.. Lowell Observatory; Estados Unidos Fil: Pelisoli, I.. Universidade Federal do Rio Grande do Sul; Brasil. University of Warwick; Reino Unido Fil: Rest, A.. Space Telescope Science Institute; Estados Unidos. University Johns Hopkins; Estados Unidos Fil: Ricci, F.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos. Universita Degli Studi Roma Tre; Italia Fil: Sako, M.. University of Pennsylvania; Estados Unidos Fil: Soares Santos, M.. Fermi National Accelerator Laboratory; Estados Unidos. Brandeis University; Estados Unidos Fil: Strader, J.. Michigan State University; Estados Unidos
description	We present optical and ultraviolet spectra of the first electromagnetic counterpart to a gravitational-wave (GW) source, the binary neutron star merger GW170817. Spectra were obtained nightly between 1.5 and 9.5 days post-merger, using the Southern Astrophysical Research and Magellan telescopes; the UV spectrum was obtained with the Hubble Space Telescope at 5.5 days. Our data reveal a rapidly fading blue component (T ≈ 5500 K at 1.5 days) that quickly reddens; spectra later than ≳4.5 days peak beyond the optical regime. The spectra are mostly featureless, although we identify a possible weak emission line at ∼7900 Å; at t ≲ 4.5 days. The colors, rapid evolution, and featureless spectrum are consistent with a "blue" kilonova from polar ejecta comprised mainly of light r-process nuclei with atomic mass number A ≲ 140. This indicates a sightline within θobs ≲ 45° of the orbital axis. Comparison to models suggests ∼0.03 M o of blue ejecta, with a velocity of . The required lanthanide fraction is ∼10-4, but this drops to <10-5in the outermost ejecta. The large velocities point to a dynamical origin, rather than a disk wind, for this blue component, suggesting that both binary constituents are neutron stars (as opposed to a binary consisting of a neutron star and a black hole). For dynamical ejecta, the high mass favors a small neutron star radius of ≲12 km. This mass also supports the idea that neutron star mergers are a major contributor to r-process nucleosynthesis.
publishDate	2017
dc.date.none.fl_str_mv	2017-10
dc.type.none.fl_str_mv	info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo
format	article
status_str	publishedVersion
dc.identifier.none.fl_str_mv	http://hdl.handle.net/11336/56893 Nicholl, M.; Berger, E.; Kasen, D.; Metzger, B. D.; Elias, J.; et al.; The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta; Institute of Physics Publishing; Astrophysical Journal Letters; 848; 2; 10-2017; 1-8 2041-8213 CONICET Digital CONICET
url	http://hdl.handle.net/11336/56893
identifier_str_mv	Nicholl, M.; Berger, E.; Kasen, D.; Metzger, B. D.; Elias, J.; et al.; The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta; Institute of Physics Publishing; Astrophysical Journal Letters; 848; 2; 10-2017; 1-8 2041-8213 CONICET Digital CONICET
dc.language.none.fl_str_mv	eng
language	eng
dc.relation.none.fl_str_mv	info:eu-repo/semantics/altIdentifier/doi/10.3847/2041-8213/aa9029 info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.3847/2041-8213/aa9029/meta
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dc.publisher.none.fl_str_mv	Institute of Physics Publishing
publisher.none.fl_str_mv	Institute of Physics Publishing
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repository.mail.fl_str_mv	dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta

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